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Planetary nebula luminosity function distances for 19 galaxies observed by PHANGS–MUSE

Scheuermann, Fabian and Kreckel, Kathryn and Anand, Gagandeep S. and Blanc, Guillermo A. and Congiu, Enrico and Santoro, Francesco and Van Dyk, Schuyler D. and Barnes, Ashley T. and Bigiel, Frank and Glover, Simon C. O. and Groves, Brent and Klessen, Ralf S. and Kruijssen, J. M. Diederik and Rosolowsky, Erik and Schinnerer, Eva and Schruba, Andreas and Watkins, Elizabeth J. and Williams, Thomas G. (2022) Planetary nebula luminosity function distances for 19 galaxies observed by PHANGS–MUSE. Monthly Notices of the Royal Astronomical Society, 511 (4). pp. 6087-6109. ISSN 0035-8711. doi:10.1093/mnras/stac110. https://resolver.caltech.edu/CaltechAUTHORS:20220427-406347100

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Abstract

We provide new planetary nebula luminosity function (PNLF) distances to 19 nearby spiral galaxies that were observed with VLT/MUSE by the PHANGS collaboration. Emission line ratios are used to separate planetary nebulae (PNe) from other bright [OIII][OIII] emitting sources like compact supernovae remnants (SNRs) or H II regions. While many studies have used narrowband imaging for this purpose, the detailed spectral line information provided by integral field unit (IFU) spectroscopy grants a more robust way of categorizing different [OIII] emitters. We investigate the effects of SNR contamination on the PNLF and find that we would fail to classify all objects correctly, when limited to the same data narrowband imaging provides. However, the few misclassified objects usually do not fall on the bright end of the luminosity function, and only in three cases does the distance change by more than 1σ. We find generally good agreement with literature values from other methods. Using metallicity constraints that have also been derived from the same IFU data, we revisit the PNLF zero-point calibration. Over a range of 8.34 < 12 + log (O/H) < 8.59, our sample is consistent with a constant zero-point and yields a value of M∗ = −4.542^(+0.103)_(−0.059) mag⁠, within 1σ of other literature values. MUSE pushes the limits of PNLF studies and makes galaxies beyond 20Mpc accessible for this kind of analysis. This approach to the PNLF shows great promise for leveraging existing archival IFU data on nearby galaxies.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.1093/mnras/stac110DOIArticle
https://arxiv.org/abs/2201.04641arXivDiscussion Paper
https://github.com/fschmnn/pnlfRelated ItemCode
ORCID:
AuthorORCID
Scheuermann, Fabian0000-0003-2707-4678
Kreckel, Kathryn0000-0001-6551-3091
Anand, Gagandeep S.0000-0002-5259-2314
Blanc, Guillermo A.0000-0003-4218-3944
Congiu, Enrico0000-0002-8549-4083
Santoro, Francesco0000-0002-6363-9851
Van Dyk, Schuyler D.0000-0001-9038-9950
Barnes, Ashley T.0000-0003-0410-4504
Bigiel, Frank0000-0003-0166-9745
Glover, Simon C. O.0000-0001-6708-1317
Groves, Brent0000-0002-9768-0246
Klessen, Ralf S.0000-0002-0560-3172
Kruijssen, J. M. Diederik0000-0002-8804-0212
Rosolowsky, Erik0000-0002-5204-2259
Schinnerer, Eva0000-0002-3933-7677
Watkins, Elizabeth J.0000-0002-7365-5791
Williams, Thomas G.0000-0002-0012-2142
Additional Information:© 2022 The Author(s). Published by Oxford University Press on behalf of Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model). Accepted 2022 January 12. Received 2022 January 11; in original form 2021 September 14. Published: 18 January 2022. We thank the anonymous referee for the helpful comments that improved this work. This work was carried out as part of the PHANGS collaboration. Based on observations collected at the European Southern Observatory under ESO programmes 1100.B-0651, 095.C-0473, and 094.C-0623 (PHANGS–MUSE; PI Schinnerer), as well as 094.B-0321 (MAGNUM; PI Marconi), 099.B-0242, 0100.B-0116, 098.B-0551 (MAD; PI Carollo) and 097.B-0640 (TIMER; PI Gadotti). FS and KK gratefully acknowledges funding from the German Research Foundation (DFG) in the form of an Emmy Noether Research Group (grant number KR4598/2-1, PI Kreckel). GA acknowledges support from the IPAC Visiting Graduate Fellowship programme and from an award from the Space Telescope Science Institute in support of programme SNAP-15922. FS, ES and TGW acknowledge funding from the ERC under the European Union’s Horizon 2020 research and innovation programme (grant agreement no. 694343). ATB and FB would like to acknowledge funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement No. 726384/Empire). SCOG and RSK acknowledge support from the DFG via SFB 881 ‘The Milky Way System’ (project-ID 138713538; subprojects A1, B1, B2, and B8) and from the Heidelberg cluster of excellence EXC 2181-390900948 ‘STRUCTURES: A unifying approach to emergent phenomena in the physical world, mathematics, and complex data’, funded by the German Excellence Strategy. RSK also thanks for support from the European Research Council via the ERC Synergy Grant ‘ECOGAL – Understanding our Galactic ecosystem: From the disc of the Milky Way to the formation sites of stars and planets’ (contract number 855130). JMDK gratefully acknowledges funding from the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) through an Emmy Noether Research Group (grant number KR4801/1-1) and the DFG Sachbeihilfe (grant number KR4801/2-1), as well as from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme via the ERC Starting Grant MUSTANG (grant agreement number 714907). ER acknowledges the support of the Natural Sciences and Engineering Research Council of Canada (NSERC), funding reference number RGPIN-2017-03987. EW acknowledges support from the DFG via SFB 881 ‘The Milky Way System’ (project-ID 138713538; subproject P2). This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. It also made use of a number of python packages, namely PHOTUTILS, an Astropy package for detection and photometry of astronomical sources (Bradley et al. 2019) as well as the main ASTROPY package (Astropy Collaboration 2013, 2018), NUMPY (Harris et al. 2020) and MATPLOTLIB (Hunter 2007). Data Availability: The MUSE data underlying this article are presented in Emsellem et al. (2021) and are available at the ESO archive. The catalogue with the planetary nebulae identifications is available in the online supplementary material of the journal. The code for this project is available at https://github.com/fschmnn/pnlf.
Group:Infrared Processing and Analysis Center (IPAC)
Funders:
Funding AgencyGrant Number
Deutsche Forschungsgemeinschaft (DFG)KR4598/2-1
Infrared Processing and Analysis Center (IPAC)UNSPECIFIED
NASASNAP-15922
European Research Council (ERC)694343
European Research Council (ERC)726384
Deutsche Forschungsgemeinschaft (DFG)SFB 881
Deutsche Forschungsgemeinschaft (DFG)138713538
Deutsche Forschungsgemeinschaft (DFG)EXC 2181-390900948
European Research Council (ERC)855130
Deutsche Forschungsgemeinschaft (DFG)KR4801/1-1
Deutsche Forschungsgemeinschaft (DFG)KR4801/2-1
European Research Council (ERC)714907
Natural Sciences and Engineering Research Council of Canada (NSERC)RGPIN-2017-03987
Subject Keywords:galaxies: distances and redshifts –ISM: supernova remnant –planetary nebulae: general
Issue or Number:4
DOI:10.1093/mnras/stac110
Record Number:CaltechAUTHORS:20220427-406347100
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20220427-406347100
Official Citation:Fabian Scheuermann, Kathryn Kreckel, Gagandeep S Anand, Guillermo A Blanc, Enrico Congiu, Francesco Santoro, Schuyler D Van Dyk, Ashley T Barnes, Frank Bigiel, Simon C O Glover, Brent Groves, Ralf S Klessen, J M Diederik Kruijssen, Erik Rosolowsky, Eva Schinnerer, Andreas Schruba, Elizabeth J Watkins, Thomas G Williams, Planetary nebula luminosity function distances for 19 galaxies observed by PHANGS–MUSE, Monthly Notices of the Royal Astronomical Society, Volume 511, Issue 4, April 2022, Pages 6087–6109, https://doi.org/10.1093/mnras/stac110
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:114485
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:27 Apr 2022 19:27
Last Modified:27 Apr 2022 19:27

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